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6 results on '"Seager, S [0000-0002-6892-6948]"'

1. TOI-4010: A System of Three Large Short-Period Planets With a Massive Long-Period Companion

Author

Kunimoto, Michelle, Vanderburg, Andrew, Huang, Chelsea X., Davis, M. Ryleigh, Affer, Laura, Cameron, Andrew Collier, Charbonneau, David, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martnez, Ghedina, Adriano, Haywood, R. D., Lienhard, Florian, López-Morales, Mercedes, Mayor, Michel, Pepe, Francesco, Pinamonti, Matteo, Poretti, Ennio, Maldonado, Jesús, Rice, Ken, Sozzetti, Alessandro, Wilson, Thomas G., Udry, Stéphane, Baptista, Jay, Barkaoui, Khalid, Becker, Juliette, Benni, Paul, Bieryla, Allyson, Bosch-Cabot, Pau, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Evans, Elise, Dupuy, Trent J., Goliguzova, Maria V., Guerra, Pere, Kraus, Adam, Lissauer, Jack J., Huber, Daniel, Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Safonov, Boris S., Schwarz, Richard P., Shporer, Avi, Stassun, Keivan G., Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua, Essack, Zahra, Lewis, Hannah M., Rose, Mark E., Kunimoto, M [0000-0001-9269-8060], Vanderburg, A [0000-0001-7246-5438], Huang, CX [0000-0003-0918-7484], Davis, MR [0000-0002-7451-4704], Affer, L [0000-0001-5600-3778], Cameron, AC [0000-0002-8863-7828], Charbonneau, D [0000-0002-9003-484X], Cosentino, R [0000-0003-1784-1431], Damasso, M [0000-0001-9984-4278], Dumusque, X [0000-0002-9332-2011], Fiorenzano, AFM [0000-0002-4272-4272], Ghedina, A [0000-0003-4702-5152], Haywood, RD [0000-0001-9140-3574], Lienhard, F [0000-0003-4047-0771], López-Morales, M [0000-0003-3204-8183], Mayor, M [0000-0002-9352-5935], Pepe, F [0000-0002-9815-773X], Pinamonti, M [0000-0002-4445-1845], Poretti, E [0000-0003-1200-0473], Maldonado, J [0000-0002-2218-5689], Rice, K [0000-0002-6379-9185], Sozzetti, A [0000-0002-7504-365X], Wilson, TG [0000-0001-8749-1962], Udry, S [0000-0001-7576-6236], Baptista, J [0000-0002-9306-1704], Barkaoui, K [0000-0003-1464-9276], Becker, J [0000-0002-7733-4522], Benni, P [0000-0001-6981-8722], Bieryla, A [0000-0001-6637-5401], Bosch-Cabot, P [0000-0002-1514-5558], Ciardi, DR [0000-0002-5741-3047], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Dupuy, TJ [0000-0001-9823-1445], Goliguzova, MV [0000-0003-2228-7914], Guerra, P [0000-0002-4308-2339], Kraus, A [0000-0001-9811-568X], Lissauer, JJ [0000-0001-6513-1659], Huber, D [0000-0001-8832-4488], Murgas, F [0000-0001-9087-1245], Palle, E [0000-0003-0987-1593], Quinn, SN [0000-0002-8964-8377], Safonov, BS [0000-0003-1713-3208], Schwarz, RP [0000-0001-8227-1020], Shporer, A [0000-0002-1836-3120], Stassun, KG [0000-0002-3481-9052], Jenkins, JM [0000-0002-4715-9460], Latham, DW [0000-0001-9911-7388], Ricker, GR [0000-0003-2058-6662], Seager, S [0000-0002-6892-6948], Vanderspek, R [0000-0001-6763-6562], Winn, J [0000-0002-4265-047X], Essack, Z [0000-0002-2482-0180], Lewis, HM [0000-0002-7871-085X], Rose, ME [0000-0003-4724-745X], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
MCC, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanets, Exoplanet dynamics, FOS: Physical sciences, DAS, 5109 Space Sciences, Hot Neptunes, QB Astronomy, Transit photometry, Exoplanet systems, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

We report the confirmation of three exoplanets transiting TOI-4010 (TIC-352682207), a metal-rich K dwarf observed by TESS in Sectors 24, 25, 52, and 58. We confirm these planets with HARPS-N radial velocity observations and measure their masses with 8 - 12% precision. TOI-4010 b is a sub-Neptune ($P = 1.3$ days, $R_{p} = 3.02_{-0.08}^{+0.08}~R_{\oplus}$, $M_{p} = 11.00_{-1.27}^{+1.29}~M_{\oplus}$) in the hot Neptune desert, and is one of the few such planets with known companions. Meanwhile, TOI-4010 c ($P = 5.4$ days, $R_{p} = 5.93_{-0.12}^{+0.11}~R_{\oplus}$, $M_{p} = 20.31_{-2.11}^{+2.13}~M_{\oplus}$) and TOI-4010 d ($P = 14.7$ days, $R_{p} = 6.18_{-0.14}^{+0.15}~R_{\oplus}$, $M_{p} = 38.15_{-3.22}^{+3.27}~M_{\oplus}$) are similarly-sized sub-Saturns on short-period orbits. Radial velocity observations also reveal a super-Jupiter-mass companion called TOI-4010 e in a long-period, eccentric orbit ($P \sim 762$ days and $e \sim 0.26$ based on available observations). TOI-4010 is one of the few systems with multiple short-period sub-Saturns to be discovered so far., Comment: 26 pages, 16 figures, published in AJ; (v3) added missing citation

Published
2023
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2. A nearby transiting rocky exoplanet that is suitable for atmospheric investigation

Author

Carlos Cifuentes, J. P. de Leon, Richard P. Schwarz, Joshua N. Winn, Hannu Parviainen, Christopher E. Henze, Thomas Henning, M. Lafarga, Courtney D. Dressing, Martin Kürster, Jorge Sanz-Forcada, Roland Vanderspek, A. Kaminski, Andreas Schweitzer, David W. Latham, Don Pollacco, Guillem Anglada-Escudé, Benjamin T. Montet, Eric L. N. Jensen, P. J. Amado, Jacob L. Bean, Ignasi Ribas, A. Fukui, P. Bluhm, C. Rodríguez López, Sara Seager, Enric Palle, Stefan Dreizler, Víctor J. S. Béjar, E. Esparza-Borges, Andrew W. Mann, Michael Fausnaugh, Rafael Luque, M. Stangret, Jose A. Caballero, Andreas Seifahrt, S. Stock, M. Cortés-Contreras, Karan Molaverdikhani, D. Montes, Núria Casasayas-Barris, Juan Carlos Morales, George R. Ricker, Artie P. Hatzes, Karen A. Collins, Thiam-Guan Tan, Felipe Murgas, Kevin I. Collins, Joseph D. Twicken, Enrique Herrero, Norio Narita, Avi Shporer, Mathias Zechmeister, Trifon Trifonov, Thomas Barclay, P. Tenenbaum, Dennis L. Kasper, Ansgar Reiners, Mahmoudreza Oshagh, Jon M. Jenkins, Julian Stürmer, Coel Hellier, Andreas Quirrenbach, Diana Kossakowski, Néstor Espinoza, V. M. Passegger, Samuel N. Quinn, S. V. Jeffers, M. Azzaro, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Trifonov, T. [0000-0002-0236-775X], Caballero, J. A. [0000-0002-7349-1387], Morales, J. C. [0000-0003-0061-518X], Seifahrt, A. [0000-0003-4526-3747], Ribas, I. [0000-0002-6689-0312], Bean, J. [0000-0003-4733-6532], Luque, R. [0000-0002-4671-2957], Parviainen, H. [0000-0001-5519-1391], Pallé, E. [0000-0003-0987-1593], Stock, S. [0000-0002-1166-9338], Zechmeister, M. [0000-0002-6532-4378], Amado, P. J. [0000-0002-8388-6040], Anglada Escudé, G. [0000-0002-3645-5977], Azzaro, M. [0000-0002-1317-0661], Barclay, T. [0000-0001-7139-2724], Béjar, V. J. S. [0000-0002-5086-4232], Bluhm, P. [0000-0002-0374-8466], Casasayas Barris, N. [0000-0002-2891-8222], Cifuentes, C. [0000-0003-1715-5087], Collins, K. A. [0000-0001-6588-9574], Collins, K. I. [0000-0003-2781-3207], Cortés Contreras, M. [0000-0003-3734-9866], Dreizler, S. [0000-0001-6187-5941], Dressing, C. D. [0000-0001-8189-0233], Esparza Borges, E. [0000-0002-2341-3233], Espinoza, N. [0000-0001-9513-1449], Fausnaugh, M. [0000-0002-9113-7162], Fukui, A. [0000-0002-4909-5763], Hatzes, A. P. [0000-0002-3404-8358], Hellier, C. [0000-0002-3439-1439], Henning, T. [0000-0002-1493-300X], Herrero, E. [0000-0001-8602-6639], Jeffers, S. V. [0000-0003-2490-4779], Jenkins, J. M. [0000-0002-4715-9460], Jensen, E. L. N. [0000-0002-4625-7333], Kaminski, A. [0000-0003-0203-8208], Kasper, D. [0000-0003-0534-6388], Kossakowski, D. [0000-0002-0436-7833], Lafarga, M. [0000-0002-8815-9416], Latham, D. W. [0000-0001-9911-7388], Mann, A. W. [0000-0003-3654-1602], Molaverdikhani, K. [0000-0002-0502-0428], Montes, D. [0000-0002-7779-238X], Montet, B. T. [0000-0001-7516-8308], Murgas, F. [0000-0001-9087-1245], Narita, N. [0000-0001-8511-2981], Oshagh, M. [0000-0002-0715-8789], Passegger, V. M. [0000-0002-8569-7243], Pollacco, D. [0000-0001-9850-9697], Quinn, S. N. [0000-0002-8964-8377], Rodríguez López, C. [0000-0001-5559-7850], Sanz Forcada, J. [0000-0002-1600-7835], Schwarz, R. P. [0000-0001-8227-1020], Schweitzer, A. [0000-0002-1624-0389], Seager, S. [0000-0002-6892-6948], Stangret, M. [0000-0002-1812-8024], Stürmer, J. [0000-0002-4410-4712], Tan, T. G. [0000-0001-5603-6895], Tenenbaum, P. [0000-0002-1949-4720], Twicken, J. D. [0000-0002-6778-7552], Vanderspek, R. [0000-0001-6763-6562], Winn, J. N. [0000-0002-4265-047X], Deutsche Forschungsgemeinschaft (DFG), Agencia Estatal de Investigación (AEI), National Aeronautics and Space Administration (NASA), European Research Council (ERC), Japan Society for the Promotion of Science (JSPS), La Caixa, Japan Science and Technology Agency (JST), German Research Foundation, Ministerio de Ciencia e Innovación (España), European Commission, National Aeronautics and Space Administration (US), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Japan Science and Technology Agency, and Ministry of Education, Culture, Sports, Science and Technology (Japan)

Subjects
Astrofísica, 010504 meteorology & atmospheric sciences, Red dwarf, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Q1, 01 natural sciences, 7. Clean energy, Physics::Geophysics, Planet, 0103 physical sciences, QB460, Transit (astronomy), 010303 astronomy & astrophysics, QB600, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Multidisciplinary, Astronomy, Orbital period, Light curve, Exoplanet, Astronomía, Radial velocity, 13. Climate action, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Spectroscopy of transiting exoplanets can be used to investigate their atmospheric properties and habitability. Combining radial velocity (RV) and transit data provides additional information on exoplanet physical properties. We detect a transiting rocky planet with an orbital period of 1.467 days around the nearby red dwarf star Gliese 486. The planet Gliese 486 b is 2.81 Earth masses and 1.31 Earth radii, with uncertainties of 5%, as determined from RV data and photometric light curves. The host star is at a distance of ~8.1 parsecs, has a J-band magnitude of ~7.2, and is observable from both hemispheres of Earth. On the basis of these properties and the planet's short orbital period and high equilibrium temperature, we show that this terrestrial planet is suitable for emission and transit spectroscopy. © 2021 American Association for the Advancement of Science. All rights reserved., Funding was provided by Deutsche Forschungsgemeinschaft through research unit FOR2544 "Blue Planets around Red Stars" and priority program SPP1992 "Exploring the Diversity of Extrasolar Planets"; Agencia Estatal de Investigacion of the Ministerio de Ciencia e Innovacion and the European Regional Development Fund through projects PID2019-109522GB-C51/2/3/4, PGC2018-098153-B-C33, SEV-2017-0709, MDM-2017-0737, AYA2016-79425-C3-1/2/3-P, ESP2016-80435-C2-1-R, and SEV-2015-0548; Klaus Tschira Stiftung; European Union's Horizon 2020 through Marie Sklodowska Curie grant 713673; "la Caixa" through INPhINT grant LCF/BQ/IN17/1162033; NASA through grants NNX17AG24G, 80NSSC19K0533, 80NSSC19K1721, and 80NSSC18K158 and the NASA Science Mission Directorate; Japan Society for the Promotion of Science KAKENHI through grants JP17H04574, JP18H01265, and JP18H05439; and Japan Science and Technology Agency PRESTO through grant JPMJPR1775.

Published
2021

3. TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

Author

Gilbert A. Esquerdo, Walter Boschin, Lars A. Buchhave, Allyson Bieryla, Karen A. Collins, Eric L. N. Jensen, Nobuhiko Kusakabe, David F. Phillips, Chelsea X. Huang, Jack J. Lissauer, Steve B. Howell, Norio Narita, E. Girardin, Christopher A. Watson, Enric Palle, Damien Ségransan, R. D. Haywood, P. Guerra, David W. Latham, S. Giacalone, Jonathan Irwin, Avi Shporer, Keivan G. Stassun, Giampaolo Piotto, E. Esparza-Borges, Gloria Andreuzzi, Felipe Murgas, Marco Pedani, Francesco Pepe, Mercedes Lopez-Morales, Scott McDermott, Courtney D. Dressing, Robert Massey, Motohide Tamura, George R. Ricker, Annelies Mortier, Giuseppina Micela, Jessie L. Christiansen, Emilio Molinari, Pau Bosch-Cabot, Jon M. Jenkins, Roland Vanderspek, Aldo F. M. Fiorenzano, Samuel N. Quinn, Hannu Parviainen, Ken Rice, Avet Harutyunyan, Akihiko Fukui, Sara Seager, Elisa V. Quintana, Massimo Cecconi, Mark E. Rose, R. Cloutier, Luca Di Fabrizio, Joshua N. Winn, Alessandro Sozzetti, Arjun B. Savel, Andrew Collier Cameron, David Charbonneau, Rachel A. Matson, Michel Mayor, Dimitar Sasselov, Christophe Lovis, Stéphane Udry, Gábor Fűrész, Xavier Dumusque, Cloutier, R [0000-0001-5383-9393], Charbonneau, D [0000-0002-9003-484X], Stassun, KG [0000-0002-3481-9052], Murgas, F [0000-0001-9087-1245], Mortier, A [0000-0001-7254-4363], Massey, R [0000-0001-8879-7138], Lissauer, JJ [0000-0001-6513-1659], Latham, DW [0000-0001-9911-7388], Haywood, RD [0000-0001-9140-3574], Guerra, P [0000-0002-4308-2339], Giacalone, SA [0000-0002-8965-3969], Bieryla, A [0000-0001-6637-5401], Winn, J [0000-0002-4265-047X], Watson, CA [0000-0002-9718-3266], Vanderspek, R [0000-0001-6763-6562], Udry, S [0000-0001-7576-6236], Tamura, M [0000-0002-6510-0681], Sozzetti, A [0000-0002-7504-365X], Shporer, A [0000-0002-1836-3120], Ségransan, D [0000-0003-2355-8034], Seager, S [0000-0002-6892-6948], Savel, AB [0000-0002-2454-768X], Sasselov, D [0000-0001-7014-1771], Rose, M [0000-0003-4724-745X], Ricker, G [0000-0003-2058-6662], Rice, K [0000-0002-6379-9185], Quintana, EV [0000-0003-1309-2904], Quinn, SN [0000-0002-8964-8377], Piotto, G [0000-0002-9937-6387], Phillips, D [0000-0001-5132-1339], Pedani, M [0000-0002-5752-6260], Parviainen, H [0000-0001-5519-1391], Palle, E [0000-0003-0987-1593], Narita, N [0000-0001-8511-2981], Molinari, E [0000-0002-1742-7735], Micela, G [0000-0002-9900-4751], Mayor, M [0000-0002-9352-5935], Matson, RA [0000-0001-7233-7508], López-Morales, M [0000-0003-3204-8183], Kusakabe, N [0000-0001-9194-1268], Jensen, ELN [0000-0002-4625-7333], Jenkins, JM [0000-0002-4715-9460], Huang, CX [0000-0003-0918-7484], Howell, SB [0000-0002-2532-2853], Fukui, A [0000-0002-4909-5763], Esquerdo, GA [0000-0002-9789-5474], Esparza-Borges, E [0000-0002-2341-3233], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Collins, KA [0000-0001-6588-9574], Cameron, AC [0000-0002-8863-7828], Christiansen, JL [0000-0002-8035-4778], Buchhave, LA [0000-0003-1605-5666], Boschin, W [0000-0001-9978-9109], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Physics, Earth and Planetary Astrophysics (astro-ph.EP), Radial velocity, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Radius, 3rd-DAS, Sitting, Exoplantet strcuture, QC Physics, Space and Planetary Science, Planet, astro-ph.EP, Period (geology), QB Astronomy, Planetary system formation, Low mass stars, Astrophysics::Earth and Planetary Astrophysics, Transit photometry, QC, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

Studies of close-in planets orbiting M dwarfs have suggested that the M dwarf radius valley may be well-explained by distinct formation timescales between enveloped terrestrials, and rocky planets that form at late times in a gas-depleted environment. This scenario is at odds with the picture that close-in rocky planets form with a primordial gaseous envelope that is subsequently stripped away by some thermally-driven mass loss process. These two physical scenarios make unique predictions of the rocky/enveloped transition's dependence on orbital separation such that studying the compositions of planets within the M dwarf radius valley may be able to establish the dominant physics. Here, we present the discovery of one such keystone planet: the ultra-short period planet TOI-1634 b ($P=0.989$ days, $F=121 F_{\oplus}$, $r_p = 1.790^{+0.080}_{-0.081} R_{\oplus}$) orbiting a nearby M2 dwarf ($K_s=8.7$, $R_s=0.45 R_{\odot}$, $M_s=0.50 M_{\odot}$) and whose size and orbital period sit within the M dwarf radius valley. We confirm the TESS-discovered planet candidate using extensive ground-based follow-up campaigns, including a set of 32 precise radial velocity measurements from HARPS-N. We measure a planetary mass of $4.91^{+0.68}_{-0.70} M_{\oplus}$, which makes TOI-1634 b inconsistent with an Earth-like composition at $5.9\sigma$ and thus requires either an extended gaseous envelope, a large volatile-rich layer, or a rocky portion that is not dominated by iron and silicates to explain its mass and radius. The discovery that the bulk composition of TOI-1634 b is inconsistent with that of the Earth favors the gas-depleted formation mechanism to explain the emergence of the radius valley around M dwarfs with $M_s\lesssim 0.5 M_{\odot}$., Comment: 27 pages, 13 figures, accepted to AAS journals. Our time series are included as a csv file in the arXiv source files

Published
2021
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4. A pair of TESS planets spanning the radius valley around the nearby mid-M dwarf LTT 3780

Author

Andrew W. Mann, Dimitar Sasselov, Jon M. Jenkins, Charles A. Beichman, Steve B. Howell, F. Lienhard, David Charbonneau, Joseph E. Rodriguez, Giampaolo Piotto, Ken Rice, Avet Harutyunyan, Matteo Pinamonti, Eric D. Lopez, Laura Kreidberg, David W. Latham, Xavier Dumusque, Mercedes Lopez-Morales, Michel Mayor, George R. Ricker, Nicola Astudillo-Defru, Jack J. Lissauer, Douglas A. Caldwell, Kevin I. Collins, A. Magazzu, Joseph D. Twicken, Joshua E. Schlieder, Andrew Collier Cameron, David F. Phillips, Xavier Delfosse, Joshua N. Winn, Dennis M. Conti, M. Stalport, Rosario Cosentino, Sara Seager, Rodrigo F. Díaz, Annelies Mortier, Sébastien Lépine, Patricia T. Boyd, Rachel A. Matson, John F. Kielkopf, David R. Ciardi, Stéphane Udry, Cesar Briceno, Thierry Forveille, Nicholas M. Law, Samuel N. Quinn, Adriano Ghedina, Lars A. Buchhave, Ennio Poretti, Nuno C. Santos, Karen A. Collins, René Doyon, Xavier Bonfils, Emilio Molinari, Aldo F. M. Fiorenzano, Jason D. Eastman, Eric L. N. Jensen, Étienne Artigau, Alessandro Sozzetti, Jonathan Irwin, Michael Vezie, Benjamin V. Rackham, Pedro Figueira, Mario Damasso, L. Mignon, Damien Ségransan, Francesco Pepe, Claudio Melo, Carl Ziegler, Jennifer G. Winters, Elisabeth Matthews, José Renan de Medeiros, Luca Di Fabrizio, Giuseppina Micela, Christophe Lovis, Ian J. M. Crossfield, François Bouchy, Christopher J. Burke, J. M. Almenara, Roland Vanderspek, John Asher Johnson, Ryan Cloutier, Peter Tenenbaum, Christopher A. Watson, Courtney D. Dressing, Robert Massey, Erica J. Gonzales, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Universidad Católica de la Santísima Concepción (UCSC), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Cloutier, R [0000-0001-5383-9393], Eastman, JD [0000-0003-3773-5142], Rodriguez, JE [0000-0001-8812-0565], Mortier, A [0000-0001-7254-4363], Pinamonti, M [0000-0002-4445-1845], Lienhard, F [0000-0003-4047-0771], Latham, DW [0000-0001-9911-7388], Collins, KA [0000-0001-6588-9574], Massey, R [0000-0001-8879-7138], Winters, JG [0000-0001-6031-9513], Charbonneau, D [0000-0002-9003-484X], Ziegler, C [0000-0002-0619-7639], Matthews, E [0000-0003-0593-1560], Kreidberg, L [0000-0003-0514-1147], Quinn, SN [0000-0002-8964-8377], Ricker, G [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Winn, J [0000-0002-4265-047X], Jenkins, JM [0000-0002-4715-9460], Udry, S [0000-0001-7576-6236], Twicken, JD [0000-0002-6778-7552], Tenenbaum, P [0000-0002-1949-4720], Sozzetti, A [0000-0002-7504-365X], Ségransan, D [0000-0003-2355-8034], Schlieder, JE [0000-0001-5347-7062], Sasselov, D [0000-0001-7014-1771], Santos, NC [0000-0003-4422-2919], Rackham, BV [0000-0002-3627-1676], Poretti, E [0000-0003-1200-0473], Piotto, G [0000-0002-9937-6387], Molinari, E [0000-0002-1742-7735], Micela, G [0000-0002-9900-4751], De Medeiros, JR [0000-0001-8218-1586], Matson, RA [0000-0001-7233-7508], Mann, AW [0000-0003-3654-1602], Magazzú, A [0000-0003-1259-4371], López-Morales, M [0000-0003-3204-8183], Lissauer, JJ [0000-0001-6513-1659], Law, N [0000-0001-9380-6457], Kielkopf, JF [0000-0003-0497-2651], Jensen, ELN [0000-0002-4625-7333], Howell, SB [0000-0002-2532-2853], Ghedina, A [0000-0003-4702-5152], Forveille, T [0000-0003-0536-4607], Figueira, P [0000-0001-8504-283X], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Díaz, RF [0000-0001-9289-5160], Conti, DM [0000-0003-2239-0567], Collins, KI [0000-0003-2781-3207], Ciardi, D [0000-0002-5741-3047], Caldwell, DA [0000-0003-1963-9616], Burke, C [0000-0002-7754-9486], Buchhave, L [0000-0003-1605-5666], Boyd, P [0000-0003-0442-4284], and Apollo - University of Cambridge Repository

Subjects
Radial velocity, 010504 meteorology & atmospheric sciences, Stellar mass, NDAS, FOS: Physical sciences, Astrophysics, M dwarf stars, 01 natural sciences, Planet, 0103 physical sciences, QB Astronomy, Spectroscopy, 010303 astronomy & astrophysics, Exoplanet systems, QC, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Radius, Planetary system, Photoevaporation, Stars, QC Physics, Space and Planetary Science, astro-ph.EP, Transit photometry, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the confirmation of two new planets transiting the nearby mid-M dwarf LTT 3780 (TIC 36724087, TOI-732, $V=13.07$, $K_s=8.204$, $R_s$=0.374 R$_{\odot}$, $M_s$=0.401 M$_{\odot}$, d=22 pc). The two planet candidates are identified in a single TESS sector and are validated with reconnaissance spectroscopy, ground-based photometric follow-up, and high-resolution imaging. With measured orbital periods of $P_b=0.77$ days, $P_c=12.25$ days and sizes $r_{p,b}=1.33\pm 0.07$ R$_{\oplus}$, $r_{p,c}=2.30\pm 0.16$ R$_{\oplus}$, the two planets span the radius valley in period-radius space around low mass stars thus making the system a laboratory to test competing theories of the emergence of the radius valley in that stellar mass regime. By combining 63 precise radial-velocity measurements from HARPS and HARPS-N, we measure planet masses of $m_{p,b}=2.62^{+0.48}_{-0.46}$ M$_{\oplus}$ and $m_{p,c}=8.6^{+1.6}_{-1.3}$ M$_{\oplus}$, which indicates that LTT 3780b has a bulk composition consistent with being Earth-like, while LTT 3780c likely hosts an extended H/He envelope. We show that the recovered planetary masses are consistent with predictions from both photoevaporation and from core-powered mass loss models. The brightness and small size of LTT 3780, along with the measured planetary parameters, render LTT 3780b and c as accessible targets for atmospheric characterization of planets within the same planetary system and spanning the radius valley., Comment: Accepted to AJ. 8 figures, 6 tables. CSV file of the RV measurements (i.e. Table 2) are included in the source code

Published
2020
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5. TESS Hunt for Young and Maturing Exoplanets (THYME) III: a two-planet system in the 400 Myr Ursa Major Group

Author

Pa Chia Thao, Silvano Desidera, Elisabeth R. Newton, Ivan Terentev, Roland Vanderspek, Martti H. Kristiansen, Peter Tenenbaum, Aaron C. Rizzuto, Eric E. Mamajek, Andrew W. Mann, David W. Latham, George R. Ricker, Nezar Hazam Sallam, John P. Doty, Douglas A. Caldwell, Francesco Pepe, Joseph D. Twicken, George Zhou, Stephen R. Kane, Michael M. Aitken, Gabriel Murawski, Adam L. Kraus, Gilbert A. Esquerdo, Guillermo Torres, Markus Rabus, Sara Seager, Marshall C. Johnson, Annelies Mortier, Serena Benatti, Bob Massey, Robert Gagliano, Tom Jacobs, Ennio Poretti, Karen A. Collins, Jon M. Jenkins, Ana Glidden, Andrew Vanderburg, Steven Villanueva, Keighley Rockcliffe, Mackenna L. Wood, Thomas Barclay, Thomas G. Wilson, Jonathan L. Bush, Perry Berlind, Rosario Cosentino, Michelle L. Hill, Diana Dragomir, Christophe Lovis, Avet Harutyunyan, Mark Omohundro, Joshua N. Winn, Hans Martin Schwengeler, Samuel N. Quinn, Daryll LaCourse, University of St Andrews. School of Physics and Astronomy, Mann, AW [0000-0003-3654-1602], Johnson, MC [0000-0002-5099-8185], Vanderburg, A [0000-0001-7246-5438], Kraus, AL [0000-0001-9811-568X], Rizzuto, AC [0000-0001-9982-1332], Wood, ML [0000-0001-7336-7725], Bush, JL [0000-0002-9446-9250], Rockcliffe, K [0000-0003-1337-723X], Newton, ER [0000-0003-4150-841X], Latham, DW [0000-0001-9911-7388], Mamajek, EE [0000-0003-2008-1488], Zhou, G [0000-0002-4891-3517], Quinn, SN [0000-0002-8964-8377], Thao, PC [0000-0001-5729-6576], Benatti, S [0000-0002-4638-3495], Desidera, S [0000-0001-8613-2589], Mortier, A [0000-0001-7254-4363], Poretti, E [0000-0003-1200-0473], Wilson, TG [0000-0001-8749-1962], Kristiansen, MH [0000-0002-2607-138X], Gagliano, R [0000-0002-5665-1879], Jacobs, T [0000-0003-3988-3245], Lacourse, DM [0000-0002-8527-2114], Kane, SR [0000-0002-7084-0529], Hill, ML [0000-0002-0139-4756], Rabus, M [0000-0003-2935-7196], Esquerdo, GA [0000-0002-9789-5474], Collins, KA [0000-0001-6588-9574], Murawski, G [0000-0001-7809-1457], Sallam, NH [0000-0003-0614-2571], Aitken, MM [0000-0002-0169-0766], Massey, B [0000-0001-8879-7138], Ricker, GR [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Winn, JN [0000-0002-4265-047X], Jenkins, JM [0000-0002-4715-9460], Barclay, T [0000-0001-7139-2724], Caldwell, DA [0000-0003-1963-9616], Dragomir, D [0000-0003-2313-467X], Glidden, A [0000-0002-5322-2315], Tenenbaum, P [0000-0002-1949-4720], Torres, G [0000-0002-5286-0251], Twicken, JD [0000-0002-6778-7552], Villanueva, S [0000-0001-6213-8804], and Apollo - University of Cambridge Repository

Subjects
ComputerSystemsOrganization_COMPUTERSYSTEMIMPLEMENTATION, 010504 meteorology & atmospheric sciences, Exoplanet astronomy, Exoplanet evolution, Library science, FOS: Physical sciences, ComputerApplications_COMPUTERSINOTHERSYSTEMS, Astrophysics::Cosmology and Extragalactic Astrophysics, 5109 Space Sciences, 01 natural sciences, Transits, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, Stellar rotation, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, Computer Science::Databases, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Stellar activity, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanet dynamics, Astronomy and Astrophysics, 3rd-DAS, Exoplanet, Young star clusters, Graduate research, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 5101 Astronomical Sciences, Astrophysics::Earth and Planetary Astrophysics, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets ($, Comment: Published in AJ. Oct 19: fixed a citation issue

Published
2020
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6. An Ultra-Hot Neptune in the Neptune desert

Author

Todd C. Klaus, Jose I. Vines, Ruth Titz-Weider, Motohide Tamura, Jessie L. Christiansen, Samuel N. Quinn, M. G. Soto, J. Villasenor, Pablo Rojas, George R. Ricker, Simon R. Walker, Maximiliano Moyano, Nicolás T. Kurtovic, Sara Seager, Sean McCauliff, Maximilian N. Günther, Andrés Jordán, Juan Cabrera, Pascal Torres, Michael R. Goad, Jerome de Leon, Giovanni Isopi, David R. Ciardi, Daniel Bayliss, K. I. Collins, Peter J. Wheatley, Jack J. Lissauer, Norio Narita, David W. Latham, François Bouchy, Sarah L. Casewell, Oliver Turner, Mayuko Mori, Andrea Ercolino, Cristobal Petrovich, Richard G. West, E. Foxell, Claudia Belardi, Philipp Eigmüller, James McCormac, Tom Louden, Eric D. Lopez, Liam Raynard, Benjamin F. Cooke, Edward Gillen, George W. King, Allyson Bieryla, Karen A. Collins, Matias Diaz, Heike Rauer, David J. Armstrong, Jack S. Acton, James A. G. Jackman, Don Pollacco, Anders Erikson, Néstor Espinoza, Michael Vezie, Samuel Gill, Nicholas M. Law, Carl Ziegler, Jon M. Jenkins, Edward M. Bryant, Rafael Brahm, Alexis M. S. Smith, Charles Beichman, Boris T. Gänsicke, Roland Vanderspek, Andrew W. Mann, Taku Nishiumi, Pía Cortés-Zuleta, Didier Queloz, Rosanna H. Tilbrook, Matthew J. Hooton, Louise D. Nielsen, Joshua N. Winn, Christopher J. Burke, Alexander Chaushev, Matthew R. Burleigh, Enric Palle, James S. Jenkins, Christopher E. Henze, Stéphane Udry, F. Mallia, Christopher A. Watson, Jenkins, JS [0000-0003-2733-8725], Espinoza, N [0000-0001-9513-1449], Brahm, R [0000-0002-9158-7315], Cortés-Zuleta, P [0000-0002-6174-4666], Wheatley, PJ [0000-0003-1452-2240], Winn, JN [0000-0002-4265-047X], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Bieryla, A [0000-0001-6637-5401], Christiansen, JL [0000-0002-8035-4778], Mori, M [0000-0003-1368-6593], Narita, N [0000-0001-8511-2981], Nishiumi, T [0000-0003-1510-8981], Tamura, M [0000-0002-6510-0681], Lissauer, JJ [0000-0001-6513-1659], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Armstrong, DJ [0000-0002-5080-4117], Bayliss, D [0000-0001-6023-1335], Cabrera, J [0000-0001-6653-5487], Casewell, SL [0000-0003-2478-0120], Eigmüller, P [0000-0003-4096-0594], Günther, MN [0000-0002-3164-9086], Hooton, MJ [0000-0003-0030-332X], Queloz, D [0000-0002-3012-0316], Smith, AMS [0000-0002-2386-4341], Udry, S [0000-0001-7576-6236], Watson, CA [0000-0002-9718-3266], West, RG [0000-0001-6604-5533], and Apollo - University of Cambridge Repository

Subjects
Extrasolare Planeten und Atmosphären, Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, 010504 meteorology & atmospheric sciences, Leitungsbereich PF, Library science, FOS: Physical sciences, Astronomy and Astrophysics, Northern ireland, 01 natural sciences, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Political science, 0103 physical sciences, astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Research center, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, QB, Astrophysics - Earth and Planetary Astrophysics
Abstract

About one out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultra-short-period planet (Sanchis-ojeda et al. 2014; Winn et al. 2018). All of the previously known ultra-short-period planets are either hot Jupiters, with sizes above 10 Earth radii (Re), or apparently rocky planets smaller than 2 Re. Such lack of planets of intermediate size (the "hot Neptune desert") has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here, we report the discovery of an ultra-short-period planet with a radius of 4.6 Re and a mass of 29 Me, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite (Ricker et al. 2015) revealed transits of the bright Sun-like star \starname\, every 0.79 days. The planet's mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0^(+2.7)_(-2.9)% of the total mass. With an equilibrium temperature around 2000 K, it is unclear how this "ultra-hot Neptune" managed to retain such an envelope. Follow-up observations of the planet's atmosphere to better understand its origin and physical nature will be facilitated by the star's brightness (Vmag=9.8)., Comment: 26 pages, 10 figures, 3 tables. Published in Nature Astronomy (21/09/2020)

Published
2020
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